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    {\small\rm\zihao{6}\songti\thepage\hfill
    \quad\quad ACTA ASTRONOMICA SINICA \hfill
    \hspace{2mm} Vol.44\vspace{2mm}}}} %%%%%%%
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    {\small\rm \zihao{6}\songti suppl.\hfill K. F. Sun et al.: High-Velocity Gas Near S106  %%（作者：题目名称）
    \vspace{1.5mm}
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\zihao{5}\songti

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    \zihao{6}\songti
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    Vol.44~ Suppl.
    \hfill\hspace{8mm} %%% if ``October/January'' then \hspace{8/10 mm} July
    \small ACTA ASTRONOMICA SINICA
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      Feb.,~2003 \\[-1.5 true mm] %%January
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\vs\vs\vs \bc {\Large\bf
High-Velocity Gas Near S106    %%（文题）
%\\[1ex]
%$\!\!^*$
}

\vs\vs{\normalsize  K.F. Sun,\hs\hs Y.F. Wu \hs\&\hs L.M. Wang }  %%（本文作者）

\vs
({\footnotesize {\it School of Physics, Peking University}~ 100871}) \\%%（本文作者单位）
 (\footnotesize {\it CAS-PKU Joint Beijing Astrophysical Center, Beijing}~100871)\\

 \vs\vs
 \ec

\normalsize
\begin{quotation}

 \no{\bf A{\scriptsize\bf BSTRACT }}~~~\small
We here presented the mapping data of $^{12}$CO $J=1-0$ and found
there was a complex bipolar molecular outflow, which had four red
clumps and two blue clumps. We analyzed the outflow and calculated
the parameters of it and found it was a massive outflow. From
Simbad data we found many IRS sources and masers near this region.
We drew a conclusion that S106 was a well-developed star formation
region.

 %\vn
 %\no{\bf Key words}~~  pulsar-mode  change-spectrum
\end{quotation}

%%%% 正文
 \para{\large\bf{1}~~ Introduction}

\vs\vs S106 is one of the most studied nearby regions of massive
star formation ~(Bally \& Yu 1998) located at a distance of
600\,pc
 ~(Eiroa, Elsasser \& Lahulla 1979), and has a bipolar H II
region ~(Sharpless 1959). An elongated double structure of
molecular line emission was found for HCN ~(Churchwell \& Bieging
1982), CO and its isotopes (Bally \& Scoville 1982) and NH3
~(Little et al 1979), which was interpreted as a biconical nebulae
constitute. There are two lobes of emission surround an obscured
central star.

\para{\large\bf{2}~~Observations and Results}

\vs\vs The observation of the $^{12}$CO $J=1-0$ mapping data was
carried out by the 13.7\,m radio telescope of Qinghai Observing
Station in April 2001. The $14\times17$ points maps were made
centered on S106. The grid spacing was near $1^{\prime}$, and the
integration time was 2 minutes for each position. Data were
reduced with Drawspec software package, and Winsurf was used for
analysis of the contours.

We analyzed every CO spectrum, calculated the emission intensities
and made contours for S106. We found that it has three primary
physical characteristics: the high velocity, the large measurable
extents and the bipolar structure (See Figure 1). These three
points suggest that the wings result in outflow motions rather
than rotation, turbulence or collapse (Lada 1985, Myers 1988).


The contour map of wing integrated intensity of S106, integrated
over the red wing ($4 \leq$ VLSR$ \leq 12$\,km/s) (solid) from
30\,K\,km/s to 120\,K\,km/s and the blue wing ($-13\leq$ VLSR
$\leq -3.5$\,km/s) (dashed) from 30\,K\,km/s to 120\,K\,km/s. they
increase in steps of 10\,K\,km/s. The stars represent the IRAS
sources and the triangles represent the IRS sources. There are
also two masers near IRAS20255+3712 ~(the central star), which are
lapped, so we did not mark them. The coordinates of these objects
are listed in Table 1.

\newpage\bc{\small\bf

 Table 1~~   The coordinates of Objects in the region
}\\[2mm]

\fns \tabcolsep 7mm
\begin{tabular}{ccc}
\hline\\[-3.6mm]\hline
Source Name & $\alpha(1950)$ & $\delta(1950)$\\
\hline
 IRAS20252+3717   & $20^{h}25^{m}12.0^{s}$ &  $+37^{\circ}17^{\prime}12^{\prime\prime}$\\
IRAS20255+3712   & $20^{h}25^{m}33.5^{s}$ &  $+37^{\circ}12^{\prime}50^{\prime\prime}$\\
IRAS20259+3708   & $20^{h}25^{m}59.6^{s}$ &  $+37^{\circ}08^{\prime}14^{\prime\prime}$\\
IRS1             & $20^{h}25^{m}32.2^{s}$ &  $+37^{\circ}12^{\prime}36^{\prime\prime}$\\
IRS2             & $20^{h}25^{m}32.5^{s}$ &  $+37^{\circ}13^{\prime}00^{\prime\prime}$\\
IRS3             & $20^{h}25^{m}32.8^{s}$ &  $+37^{\circ}12^{\prime}45^{\prime\prime}$\\
IRS3S            & $20^{h}25^{m}33.9^{s}$ &  $+37^{\circ}12^{\prime}47^{\prime\prime}$\\
IRS3W            & $20^{h}25^{m}33.6^{s}$ &  $+37^{\circ}12^{\prime}50^{\prime\prime}$\\
IRS4             & $20^{h}25^{m}32.8^{s}$ &  $+37^{\circ}12^{\prime}50^{\prime\prime}$\\
IRS5             & $20^{h}25^{m}33.9^{s}$ &  $+37^{\circ}12^{\prime}59^{\prime\prime}$\\
IRS6             & $20^{h}25^{m}34.1^{s}$ &  $+37^{\circ}12^{\prime}29^{\prime\prime}$\\
IRS7             & $20^{h}25^{m}34.5^{s}$ &  $+37^{\circ}12^{\prime}41^{\prime\prime}$\\
IRS8             & $20^{h}25^{m}34.9^{s}$ &  $+37^{\circ}13^{\prime}03^{\prime\prime}$\\
Maser076.36-00.60& $20^{h}25^{m}32.8^{s}$ &  $+37^{\circ}12^{\prime}54^{\prime\prime}$\\
Onsala 134       & $20^{h}25^{m}32.7^{s}$ &  $+37^{\circ}12^{\prime}54^{\prime\prime}$\\
\hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec

\begin{figure}[tbph]
\center {\includegraphics [bb= 0 0 665 760,scale=0.35]{fig1.eps}}

   \parbox[tb]{12cm}
   %{\hspace{3.5cm}
  { %\center
   \footnotesize

   Fig.\,1~~ The contour map of wing integrated intensity of S106}

    \end{figure}

There is a bipolar outflow in this region. The center of S106 is
$\alpha(1950)=20^{h}25^{m}34.0^{s},\linebreak
\delta(1950)=37^{\circ}12 ^{\prime}52^{\prime\prime}$. We can see
that the red-shifted component has four clumps: two are near the
center and the other two are marked ``red\_C'' and ``red\_D''(See
Figure 2), which are similar with the $^{13}$CO map of S106
 (Pipher et al 1970). The blue-shifted component has two
clumps:one is near the center, which is among the two red clumps;
and the other is marked ``blue\_B''(See Figure 2), which is among
the other two red clumps: ``red\_C'' and ``red\_D''.
IRAS20255+3712 is located near the center of the S106, surrounded
by one blue clump and two red clumps; IRAS20259+3708 is surrounded
by one blue clump and one red clump; IRAS20252+3717 is out of the
integrated intensity region. The reason of the complexity of this
outflow may be that the first two sources both drive their own
outflows, in other word, the clumps may come from different
outflows. The radiation of IRAS20252+371 may impact this region
and lead to the compact part near the source.

By using the method by Goldsmith et al. ~(1984), we calculated the
outflow parameters. Under the assumption of LTE and the optical
thin wing, the total column density of CO molecules can be
calculated as following:

$$ N_{\rm CO}={{4.2\times
10^{13}}\over{\exp(-5.5/T_{\rm ex})}} T_{\rm
ex}\int{T_{R}(v)dv}({\rm cm}^{-2})
$$

Here, $T_{\rm ex}$ is excited temperature and $T_{R}$ is the
radiation temperature. If we further assume a CO abundance $X_{\rm
CO}=[\rm CO]/[{\rm H}_2]=10^{-4}$, the column density of the
high-velocity gas is $N=N_{\rm CO}/{X_{\rm CO}}$. All results of
calculation are given in Table 2. Table 3 lists the parameters of
these three IRAS sources.

\bc{\small\bf

 Table 2~~   Outflow parameters
}\\[2mm]

\fns \tabcolsep 2mm
\begin{tabular}{ccccc}
\hline\\[-3.6mm]\hline
 size (pc) & V (km\,s$^{-1}$)& M (M$_{\odot}$)&
  P (M$_{\odot}$\,km\,s$^{-1}$)& E (erg)\\
0.6&    8.63&   151.92&  1312.56&   $1.09\times10^{47}$\\
\\
t (yr) &F(M$_{\odot}$\,km\,s$^{-1}$\,yr$^{-1}$)&$L_{\rm mech}$
($L_{\odot}$)&
 $M_{\rm loss}$ (M$_{\odot}$\,yr$^{-1}$)&\\
 $8.22\times10^{4}$& $1.59\times10^{-2}$& 10.8& $5.3\times 10^{-5}$&\\
 \hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec

\bc{\small\bf

 Table 3~~   Parameters of the IRAS sources
}\\[2mm]

\fns \tabcolsep 3mm
\begin{tabular}{clllll}
\hline\\[-3.6mm]\hline
 Source Name&$F_{12}$(Jy)& $F_{25}$(Jy)& $F_{60}$(Jy)& $F_{100}$(Jy)&$L_{\rm bol}$
 ($L_{\odot}$)\\
\hline
IRAS20252+3717 & 2.07 &  1.10 &   16.8 & 16.8 & 2621.74 \\
IRAS20255+3712 &  205 &  2510 &  10100 & 13100& 10693.11\\
IRAS20259+3708  & 1.26 &  5.44 &   31.0 &   113& 46.65\\
 \hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec

From these Tables, we know this outflow is middle-size one and the
bolometric luminosity of IRAS20255+3712 is 10693.11$L_{\odot}$,
which is a massive star. We compared the bolometric luminosity
with the mechanical luminosity, and found that the ratio is
990.10, which means that the radiation of the central young
stellar object (YSO) can drive the outflow.

\para{\large\bf{3}~~Summary}

\vs\vs We have observed the high-velocity $^{12}$CO gas near S106
and found the complex bipolar molecular outflow. We estimated the
parameters by using the method of Goldsmith et al ~(1984) and
found it was a middle-size molecular outflow.

\vs\vn{\bf ACKNOWLEDGEMENT}~~ This project was supported by
G1999075405 of NKBRSF, 10128306 and 10133020.

\bc {\bf References} \ec

\vspace{-4mm} \no \fns

 \nref  Eiroa C.,  Elsasser H.,  Labulla J.F., A\&A, 1979, 74: 89
\nref
 Roberts D.A., Crutcher R.M., Troland T.H., ApJ, 1995, 442: 208
\nref  Churchwell E.,  Bieging J.H., ApJ, 1982, 258: 515 \nref
Jijina J.,  Myers P.C.,  Fred  Database C., ApJS, 1999, 125: 161
 \nref  Bally J.,  Scoville N.Z., ApJ, 1982, 255: 497
\nref  Little L.T.,  Macdonald G.H.,  Riley P.W., et al, MNRAS,
1979, 188: 429 \nref  Goldsmith P.F., Snell R.L., Hemeon-Heyer M.,
et al, ApJ, 1984, 286: 599 \nref  Sharpless S., ApJS, 1959, 4: 257
\nref Wood,  Douglas O.S., Ed Churchwell, ApJ, 1989, 340: 265

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